| 2025-12-31 |
hst_1303.pmap |
latest |
The ACS WFC bias, dark, CTE dark, and sink files were generated following the ACS WFC anneal on December 21, 2025, and should be used to calibrate ACS WFC observations taken between November 17, 2025 and December 21, 2025. |
| 2025-12-29 |
hst_1302.pmap |
archived |
Delivery of new STIS CCD bias and dark reference files for CCD data taken between Nov 26 and Dec 25, 2025. The files were generated from data taken in the same time frame under STIS calibration programs 18157 and 18154. |
| 2025-12-23 |
hst_1301.pmap |
archived |
The COS team has delivered the first operational reference files for use at LP10, replacing the previous temporary LP10 reference files. The files delivered include a LAMPTAB, DISPTAB, XTRACTAB, TWOZXTAB, PROFTAB, TRACETAB, FLATFILE, and FLUXTAB. In Fall 2025, at the start of HST Cycle 33, LP10 was enabled for use with the G160M/1533, 1577, 1589, 1600, 1611, and 1623 modes. These eight reference files provide optimally calibrated data at LP10 and allows for TWOZONE extraction at LP10. |
| 2025-12-17 |
hst_1300.pmap |
archived |
These WFC3 UVIS superdarks will affect all UVIS data taken from November 11, 2025 to December 10, 2025. Currently, the automated calibration pipeline and CRDS have only WFC3 UVIS drk and dkc reference files with USEAFTER dates of up to November 9, 2025. The automated pipeline should now use these reference files to perform dark subtraction on any UVIS datasets obtained between the dates above, as they represent the most accurate picture of dark current and hot pixels for this time period. This new bad pixel table with USEAFTER of November 11, 2025 was generated using data taken from November 11, 2025, through December 13, 2025. Currently, the Calibration Reference Data System only has WFC3 UVIS bad pixel reference tables up to a USEAFTER date of October 16, 2025. The automated pipeline should now use this reference file as the bad pixel table on any UVIS datasets obtained from November 11, 2025 to present because it represents the most accurate measure of pixel stability at the time of the science observation. These WFC3 UVIS bad pixel files were generated using 900 second dark exposures from the HST Cycle 32 and 33 daily monitoring programs 17665, 17669, 17944, and 17946. More information about the UVIS bad pixel tables is outlined in the WFC3 ISR 2018.15 and WFC3 ISR 2021.14. For more details regarding both deliveries, please see the Context History and select ,all contexts, on the CRDS homepage. |